Main Objective: Studying the dynamics of the low atmosphere counterpart of the AR outflows using IRIS and SST
Scientific Justification: Strong and persistent blueshifts at the edge of active regions (so-called gactive region outflowsh) are routinely observed by EIS in the spectra of high-temperature lines such as Fe XII, and are widely considered to be a candidate source of the slow solar wind (e.g. Harra et al. 2008, Doschek et al. 2008, Brooks et al. 2011, 2012). To fully understand how these outflows are driven, which is crucial to both coronal heating and solar wind studies, we need to characterize their evolution through different layers of the solar atmosphere, from the chromosphere to the corona. We will use SST and IRIS observations to investigate the spectral properties of chromospheric and TR lines (e.g. H alpha, Ca II H/K, Mg II, CII, SI IV) at very high spatial, temporal and spectral resolution. This will allow us to obtain information on the physical conditions of the plasma, such as flows, velocity gradients and turbulence, and investigate the response of the low atmosphere counterpart of the coronal outflows. EIS observations over a broader range of temperatures will fill the gap between the TR and corona and provide measurements of flows, densities and abundances in the outflows regions. SST/CRISP will also provide high-quality Mg I magnetograms, which are crucial to understand the magnetic connectivity in these regions. |
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